4. INNER SPACE AND OUTER SPACE

The ``hot'' in the hot big-bang cosmology makes
fundamental physics an inseparable part of the
standard cosmology. The time - temperature
relation, kBT ~ 1 MeV (t/sec )-1/2,
implies that the physics of higher energies and shorter
times is required to understand the Universe
at earlier times: atomic physics at t
1013 sec, nuclear physics at t ~ 1 sec,
and elementary-particle physics at t < 10-5 sec.
The standard cosmology model itself is based upon Einstein's
general relativity, which embodies our deepest
and most accurate understanding of gravity.

The standard model of particle physics, which
is a mathematical description of
the strong, weak and electromagnetic
interactions based upon the SU(3) SU(2) U(1) gauge theory, accounts for all known
physics up to energies of about 300 GeV
(Gaillard et al. 1999).
It provides the input microphysics for the standard
cosmology necessary to discuss events as early
as 10-11 sec. It also provides a firm foundation
for speculations about the Universe at even earlier times.

A key feature of the standard model of particle
physics is asymptotic freedom: at high energies
and short distances, the interactions between the
fundamental constituents of matter - quarks and
leptons - are perturbatively weak.
This justifies approximating the early Universe
as hot gas of noninteracting particles (dilute
gas approximation) and opens the door to sensibly
speculating about times as early as 10-43 sec,
when the framework of general relativity becomes
suspect, since quantum corrections to this classical
description are expected to become important.

The importance of asymptotic freedom for early-Universe
cosmology cannot be overstated. A little more than
twenty-five years ago, before the advent of quarks and leptons
and asymptotic freedom,
cosmology hit a brick wall at 10-5 sec because
extrapolation to early times was nonsensical. The problem
was twofold: the finite size of nucleons and related
particles and the exponential rise in the number of ``elementary
particles'' with mass. At around 10-5 sec, nucleons would
be overlapping, and with no understanding of the strong forces
between them, together with the the exponentially rising spectrum
of particles, thermodynamics became ill-defined at higher
temperatures.

The standard model of particle physics has provided particle
physicists with a reasonable foundation for speculating about
physics at even shorter distances and higher energies. Their
speculations have significant cosmological implications, and -
conversely - cosmology holds the promise to test some of their
speculations. The most promising particle physics ideas (see e.g.,
Schwarz & Seiberg 1999)
and their cosmological implications are:

Spontaneous Symmetry Breaking (SSB). A key
idea, which is
not fully tested, is that most of the underlying symmetry in a
theory can be hidden because the vacuum state does not respect
the full symmetry; this is known as spontaneous symmetry breaking
and accounts for the carriers of the weak force, the
W± and Z0
bosons, being very massive. (Spontaneous symmetry breaking is
seen in many systems, e.g., a ferromagnet at low temperatures:
it is energetically favorable for the spins to align thereby
breaking rotational symmetry.)
In analogy to symmetry breaking in a ferromagnet,
spontaneously broken symmetries
are restored at high temperatures. Thus, it is likely that
the Universe underwent a phase transition at around 10-11 sec
when the symmetry of the electroweak theory was broken, SU(2)
U(1) -> U(1).

Grand unification. It is possible to unify
the strong,
weak, and electromagnetic interactions by a larger gauge group, e.g.,
SU(5), SO(10), or E8. The advantages are twofold:
the three forces are described
as different aspects of a more fundamental force with a single
coupling constant, and the quarks and leptons are unified as they
are placed in the same particle multiplets. If true, this would
imply another stage of spontaneous symmetry breaking, G ->
SU(3) SU(2) U(1). In addition, grand unified theories
(or GUTs) predict that baryon and lepton number are violated - so
that the proton is unstable and neutrinos have mass -
and that stable topological defects
associated with SSB may exist, e.g., point-like defects
called magnetic monopoles, one-dimensional defects referred to
as ``cosmic'' strings, and and two-dimensional defects called
domain walls. The cosmological implications of GUTs are manifold:
neutrinos as a dark matter component, baryon and lepton number violation
explaining the matter - antimatter asymmetry of the Universe,
and SSB phase transitions producing topological defects that
seed structure formation or a burst of tremendous expansion
called inflation.

Supersymmetry. In an attempt to put bosons
and fermions
on the same footing, as well as to better understand the
`hierarchy problem,' namely, the large gap between
the weak scale (300 GeV) and the Planck scale (1019 GeV),
particle theorists have postulated supersymmetry, the symmetry
between fermions and bosons. (Supersymmetry also appears to
have a role to play in understanding gravity.) Since the
fundamental particles of the standard model of particle physics
cannot be classified as fermion - boson pairs,
if correct, supersymmetry implies the existence of a superpartner for
every known particle, with a typical mass of order 300 GeV.
The lightest of these superpartners, is usually stable
and called ``the neutralino.''
The neutralino is an ideal dark matter candidate.

Superstrings, supergravity, and M-theory.
The unification
of gravity with the other forces of nature has long been the holy
grail of theorists. Over the past two decades there have been
some significant advances: supergravity, an 11-dimensional
version of general relativity with supersymmetry, which unifies
gravity with the other forces; superstrings,
a ten-dimensional theory of relativistic strings, which unifies
gravity with the other forces in a self-consistent, finite theory;
and M-theory, an ill-understood, ``larger'' theory that encompasses
both superstring theory and supergravity theory. An obvious
cosmological implication is the existence of additional spatial
dimensions, which today must be ``curled up'' to escape notice,
as well as the possibility of sensibly describing cosmology at times
earlier than the Planck time.

Advances in fundamental physics have been crucial to advancing
cosmology: e.g., general relativity led to the first self-consistent
cosmological models; from nuclear physics came big-bang nucleosynthesis;
and so on. The connection between fundamental physics and cosmology
seems even stronger today and makes realistic the hope that much
more of the evolution of the Universe will be explained by fundamental
theory, rather than ad hoc theory that dominated cosmology before
the 1980s. Indeed, the most promising paradigm for extending
the standard cosmology, inflation + cold dark matter, is deeply
rooted in elementary particle physics.